Linked from

The 28 pages that link to Jeans instability, each with the reason it gives.

• Stellar evolutionRelated: It describes when a cloud fragment can begin collapsing toward protostars.

• Star formationRelated: It describes when a cloud region can overcome pressure and begin collapsing.

• Molecular cloudRelated: It describes when a dense cloud region can overcome pressure and begin gravitational collapse.

• Initial mass functionRelated: Its characteristic mass scale may help explain how gas conditions influence stellar birth masses.

• Gravitational collapseRelated: It predicts when a gas cloud can begin collapsing instead of remaining pressure-supported.

• Gravitational instabilityBroader topic: It gives the classic criterion for when gas-density fluctuations grow instead of being pressure-supported.

• ProtostarRelated: It describes when a cloud region can begin collapsing toward protostellar formation.

• Molecular hydrogenRelated: Cooling by H₂ lowers gas pressure and can help a cloud become gravitationally unstable.

• Massive starRelated: Cloud collapse supplies the initial fragments from which massive stars grow.

• Density wave theoryRelated: Self-gravity can reinforce the density perturbations that make up a spiral wave.

• Cold dark matterRelated: It describes how perturbations in the dark matter distribution can grow into bound structures.

• Population III starRelated: It describes how dense primordial clouds could begin collapsing into protostars.

• NebulaRelated: Cloud regions become star-forming when gravity overcomes their internal support.

• StarRelated: It describes when a region of a molecular cloud can fragment and contract into a protostar.

• Disk instabilityRelated: Disk fragments collapse through the same competition between gravity and gas pressure.

• Dark nebulaRelated: It describes when a cloud region can begin contracting toward star formation.

• Eagle NebulaRelated: Dense knots can collapse into stars as cloud material is compressed and cools.

• Bok globuleRelated: It describes when a cold, dense globule can fragment or begin collapsing.

• Static universeRelated: It illustrates why matter in a static cosmos would tend to clump rather than remain uniform.

• Prestellar coreRelated: It describes when a prestellar core can no longer resist collapse.

• Rho Ophiuchi cloud complexRelated: It describes how dense regions within the complex can begin gravitational collapse.

• Structure formationRelated: It identifies when gas fluctuations can collapse rather than disperse.

• Interstellar cloudRelated: It estimates when a cloud region can begin collapsing despite internal pressure.

• Young stellar objectRelated: It describes when a cloud fragment can begin collapsing toward star formation.

• Astronomical masses and mass distributionsRelated: The Jeans mass identifies which gas clouds can collapse to form stars.

• Jim PeeblesRelated: It describes the basic gravitational growth process behind structure formation models.

• Stochastic self-propagating star formation modelRelated: Triggered compression can push gas toward gravitational collapse.

• Thomas Chrowder ChamberlinCompared with: It describes a different route from diffuse gas to structure than Chamberlin’s ejected-material account.